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The Impact of Quasars on Galaxy Evolution

This article explores how quasars influence gas dynamics and star formation in galaxies.

Michele Perna, Santiago Arribas, Xihan Ji, Cosimo Marconcini, Isabella Lamperti, Elena Bertola, Chiara Circosta, Francesco D'Eugenio, Hannah Übler, Torsten Böker, Roberto Maiolino, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Chris J. Willott, Giovanni Cresci, Eleonora Parlanti, Bruno Rodríguez Del Pino, Jan Scholtz, Giacomo Venturi

― 5 min read


Quasars and Their Cosmic Quasars and Their Cosmic Effects evolution through gas outflows. Examining how quasars shape galactic
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We are diving into the fascinating world of Quasars and what happens when they start blowing gas into space. Imagine a star that's super powerful, pouring out streams of gas. Sounds cool, right? Well, that’s basically what a quasar does, and it can change the environments around it.

Quasars Explained

Quasars are some of the brightest objects in the universe, powered by supermassive Black Holes at their centers. They consume gas and dust, and as they do, they shine brightly. If a quasar has a lot of material falling into it, it can start to blow gas back out into space. This outflow can affect Star Formation and the growth of black holes.

Outflows: The Quasar's Breath

Imagine a quasar as a huge cosmic vacuum cleaner. At times, it’s sucking in everything around it, but sometimes it gets too full and starts blowing everything back out. This outflow can happen in different speeds and directions, kind of like a giant burp.

Why Study Outflows?

Studying these outflows is important. Knowing how they work helps scientists understand how galaxies change over time. Just like how a sneeze can spread germs, a quasar's outflow can spread materials throughout a galaxy, influencing new star creation in the process.

The Quasar at Hand

The specific quasar we’re looking at is a Compton thick one, meaning it’s surrounded by a lot of material that makes it harder to see. It is a unique case and results in some interesting gas outflows.

How Do We Observe These Outflows?

To study this quasar, astronomers combine data from different telescopes, each observing different parts of the light spectrum. The James Webb Space Telescope (JWST) and the Very Large Telescope (VLT) are like two detectives working together to gather evidence, with one focusing on the ultraviolet light and the other on the optical light.

Digging Deeper

In our study, we find two main components of the outflow. The first part looks like a rotating disk – think of it as a galactic merry-go-round. The second part is a giant, cone-shaped outflow.

The Science Behind It

We take a close look at the various light signals coming from these gas streams. It’s like trying to piece together a puzzle, where each piece tells us something about the gas's behavior and speed.

Blowing Bubbles in Space

As the gas flows outward, it moves like bubbles rising in soda. By closely examining these bubbles, astronomers can determine how much gas is being ejected and how fast it is moving. This gives clues about the quasar's strength and activity.

The Relationship Between Outflows and Black Holes

There’s a connection between the gas outflows and the black hole at the center of the quasar. The more the black hole consumes gas, the stronger the outflow. It’s a balancing act, where too much gas could either lead to more star formation or blow everything away.

What About the Surrounding Environment?

The area surrounding the quasar plays a big role. If the outflow pushes gas away, it might prevent new stars from forming, similar to how a sharp wind can stop a seed from planting. Understanding this helps astronomers figure out the lifecycle of galaxies.

Analyzing the Data

The data collection is a bit like collecting pieces of fruit from different trees. Some fruits (data) come from the ultraviolet light, while others come from the optical range. By mixing these together, scientists are able to create a fuller picture of what’s happening in the quasar's environment.

The Galactic Dance

The ionized gas we observe is part of a cosmic ballet, where gas flows in circles and spirals around the quasar. This movement helps us observe how this gas interacts with the black hole and understand the dynamic relationship between them.

Gas and the Cosmic Environment

When the quasar ejects gas, that gas doesn't just disappear. It interacts with other materials in the galaxy and can influence whether new stars will be born or if existing ones will survive. It’s a dramatic and often chaotic process.

How Fast is It Moving?

We measure the outflow velocity to find out how quickly the gas is moving. The faster the gas, the more dramatic the scene. It’s like watching a race – the speed gives us an idea of how energetic the quasar is.

Gas Composition

The composition of the gas also matters. Different elements tell us what kind of processes are happening within the quasar and might point to how fresh or old the gas is.

The Impact on Galaxies

Quasar outflows help shape the fate of galaxies. If a quasar blows away too much gas, it could slow down or even stop new star formation, drastically changing how the galaxy evolves over millions of years.

Bringing It All Together

By studying outflows from quasars, astronomers are piecing together a grand cosmic story. Each quasar acts like a chapter in a book, with each outflow telling part of the narrative about how galaxies live, die, and live again.

Why This Matters

These studies are important not just for understanding individual quasars but for grasping the entire universe's history. Just like every breath we take is part of our life story, every outflow from a quasar contributes to the broader cosmic tale.

Future Observations

Looking ahead, astronomers will continue to observe quasars and their outflows with better technology. By improving their tools, they hope to gather even more detailed information, which is like upgrading from an old flip phone to the latest smartphone.

Conclusion: The Cosmic Symphony

In conclusion, studying quasar outflows reveals a cosmic symphony of interactions that shape galaxies over time. Each burst of gas is like a music note, contributing to a much larger melody of the universe.

So, the next time you look up at the stars, remember the quasars and their wild, energetic dance, crafting the fabric of our universe. Who knows? You might even hear them sing!

Original Source

Title: GA-NIFS: A galaxy-wide outflow in a Compton-thick mini-BAL quasar at z = 3.5 probed in emission and absorption

Abstract: Studying the distribution and properties of ionised gas in outflows driven by AGN is crucial for understanding the feedback mechanisms at play in extragalactic environments. In this study, we explore the connection between ionised outflows traced by rest-frame UV absorption and optical emission lines in GS133, a Compton thick AGN at z = 3.47. We combine observations from the JWST NIRSpec Integral Field Spectrograph (IFS) with archival VLT VIMOS long-slit spectroscopic data, as part of the GA-NIFS project. We perform a multi-component kinematic decomposition of the UV and optical line profiles to derive the physical properties of the absorbing and emitting gas in GS133. Our kinematic decomposition reveals two distinct components in the optical lines. The first component likely traces a rotating disk with a dynamical mass of 2e10 Msun. The second component corresponds to a galaxy-wide, bi-conical outflow, with a velocity of 1000 km/s and an extension of 3 kpc. The UV absorption lines show two outflow components, with bulk velocities v_out = -900 km/s and -1900 km/s, respectively. This characterises GS133 as a mini-BAL system. Balmer absorption lines with similar velocities are tentatively detected in the NIRSpec spectrum. Both photoionisation models and outflow energetics suggest that the ejected absorbing gas is located at 1-10 kpc from the AGN. We use 3D gas kinematic modelling to infer the orientation of the [O III] bi-conical outflow, and find that a portion of the emitting gas resides along our line of sight, suggesting that [O III] and absorbing gas clouds are partially mixed in the outflow. The derived mass-loading factor (i.e. the mass outflow rate divided by the SFR) of 1-10, and the kinetic coupling efficiency (i.e. the kinetic power divided by LAGN) of 0.1-1% per cent suggest that the outflow in GS133 provides significant feedback on galactic scales.

Authors: Michele Perna, Santiago Arribas, Xihan Ji, Cosimo Marconcini, Isabella Lamperti, Elena Bertola, Chiara Circosta, Francesco D'Eugenio, Hannah Übler, Torsten Böker, Roberto Maiolino, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Chris J. Willott, Giovanni Cresci, Eleonora Parlanti, Bruno Rodríguez Del Pino, Jan Scholtz, Giacomo Venturi

Last Update: 2024-11-20 00:00:00

Language: English

Source URL: https://arxiv.org/abs/2411.13698

Source PDF: https://arxiv.org/pdf/2411.13698

Licence: https://creativecommons.org/licenses/by/4.0/

Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.

Thank you to arxiv for use of its open access interoperability.

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